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3C58 in Context
Cosmic X-rays May Reveal New Form of Matter
Chandra's X-ray Image of 3C58:
Pullout box shows the inner nebula
Credit: NASA/SAO/CXC/P.Slane et al.
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3C58 is a young supernova remnant
believed to have resulted from an explosion in the year 1181 A.D.
At its center is a pulsar - a highly magnetized, rapidly rotating
neutron star. This young neutron star is embedded in extended emission
that is presumably produced by energetic particles that are accelerated
in the rotating magnetic field.
Neutron stars are born extremely hot. Although neutron stars cool very rapidly, X-radiation from the surface of a star as young as that in 3C58 should
be readily observable. However, this 820-year-old star, has apparently cooled so quickly that its X-ray emission has already faded below detectability.
Illustration of a Pulsar
Credit: NASA
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In order to set a limit on the temperature of the neutron star in 3C58, the scientists had to disentangle the possible contribution of X-rays from hot neutron star surface from the synchrotron X-rays due to high-energy electrons spiraling in the rapidly rotating magnetic field of the neutron star.
Return to RX J1856.5-3754 / 3C58
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